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We have developed a detailed standard chemical evolution model to study theevolution of all the chemical elements up to the iron peak in the solarvicinity. We consider that the Galaxy was formed through two episodes ofexponentially decreasing infall, out of extragalactic gas. In a first infallepisode, with a duration of $\sim$ 1 Gyr, the halo and the thick disk wereassembled out of primordial gas, while the thin disk formed in a second episodeof infall of slightly enriched extragalactic gas, with much longer timescale.The model nicely reproduces the main observational constraints of the solarneighborhood, and the calculated elemental abundances at the time of the solarbirth are in excellent agreement with the solar abundances. By the inclusion ofmetallicity dependent yields for the whole range of stellar masses we followthe evolution of 76 isotopes of all the chemical elements between hydrogen andzinc. Those results are confronted with a large and recent body ofobservational data, and we discuss in detail the implications for stellarnucleosynthesis.Comment: 19 pages, 14 figures, submitted to A&

Galactic chemical abundance evolution in the solar neighborhood up to the iron peak